This mass range is also close to the one found by dynamical simulations investigating the formation of water-rich and habitable planets [1]}. These mass and water content ranges have not been properly quantified so far in the literature because conventional models [2]}, [3]}, [4]} describe the internal structures of planets with thick atmospheres neglecting the combination of two important effects: i) the compression of the interior due to the weight of the hydrosphere, and ii) the possibility of atmospheric instability at low planetary masses. While the latter can be overlooked for temperate planets, it is critical for high irradiation temperatures and sub-Earth masses. To overcome this issue, we use a self-consistent model in which the atmosphere is coupled with the interior.
